Skip to main content
We gratefully acknowledge support from the Simons Foundation, member institutions, and all contributors. Donate
arXiv logo
Cornell University Logo

Astrophysics

arXiv:0706.2879 (astro-ph)
[Submitted on 20 Jun 2007]

Title:X-rays from RU Lupi - Accretion and winds in CTTS

Authors:J. Robrade, J.H.M.M. Schmitt
View PDF
Abstract: Using three XMM-Newton observations we study the X-ray emission of RU Lup, a accreting and wind-driving CTTS. In comparison with other bright CTTS we study possible signatures of accretion and winds in their X-ray emission. Results: We find three levels of activity among the observations of RU Lup, clearly of magnetic origin due to the corresponding high plasma temperatures. Density analysis with the OVII triplet indicates high densities in the cool plasma, suggesting accretion shocks to be a significant contributor to the soft X-ray emission. No strong overall metal depletion is observed. Excess emission at 6.4 keV during the more active phase suggest the presence of iron fluorescence. In accreting stars we find an excess of cool plasma as evidenced by lower OVIII/OVII line ratios compared to main-sequence stars. High density plasma appears to be only present in low-mass CTTS, while accreting stars with intermediate masses (> 2 M_Sun) have lower densities. Conclusions: In all investigated CTTS the characteristics of the cooler X-ray emitting plasma are influenced by the accretion process. We suspect different accretion rates and amount of funneling, possibly linked to stellar mass and radius, to be mainly responsible for the different properties of their cool plasma component. The exceptional strong X-ray absorption in RU Lup and other CTTS is probably related to accretion flows and an optically transparent wind emanating from the star or the disk.
Comments: accepted by A&A, 10 pages
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:0706.2879 [astro-ph]
  (or arXiv:0706.2879v1 [astro-ph] for this version)
  https://doi.org/10.48550/arXiv.0706.2879
Related DOI: https://doi.org/10.1051/0004-6361%3A20077644

Submission history

From: Jan Robrade [view email]
[v1] Wed, 20 Jun 2007 14:41:13 UTC (83 KB)
Full-text links:

Access Paper:

view license
Current browse context:
astro-ph
< prev   |   next >
new | recent | 2007-06

References & Citations

export BibTeX citation

Bookmark

BibSonomy logo Reddit logo

Bibliographic and Citation Tools

Bibliographic Explorer (What is the Explorer?)
Connected Papers (What is Connected Papers?)
Litmaps (What is Litmaps?)
scite Smart Citations (What are Smart Citations?)

Code, Data and Media Associated with this Article

alphaXiv (What is alphaXiv?)
CatalyzeX Code Finder for Papers (What is CatalyzeX?)
DagsHub (What is DagsHub?)
Gotit.pub (What is GotitPub?)
Hugging Face (What is Huggingface?)
Papers with Code (What is Papers with Code?)
ScienceCast (What is ScienceCast?)

Demos

Replicate (What is Replicate?)
Hugging Face Spaces (What is Spaces?)
TXYZ.AI (What is TXYZ.AI?)

Recommenders and Search Tools

Influence Flower (What are Influence Flowers?)
CORE Recommender (What is CORE?)
IArxiv Recommender (What is IArxiv?)

arXivLabs: experimental projects with community collaborators

arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website.

Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them.

Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.

Which authors of this paper are endorsers? | Disable MathJax (What is MathJax?)